The neutrons inside neutron stars are almost certainly superfluid below a critical temperature Tc 1010 K. Below Tc, pairs of excited neutron quasiparticles may recombine, resulting, if weak neutral currents exist, in the emission of neutrino-antineutrino pairs. We calculate the emissivity associated with this process and compare it with other neutrino emissivities. For neutron star interior temperatures in the range K the recombination emissivity can dominate all others. Subject headings: neutrinos - nuclear reactions stars: neutron
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Flowers et al. (1976) studied this question.